INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE

By B. Chandran, T. Dennis, E. Quataert, S. Bale. 2011

147 citations recorded by the source corpus.

We develop a one-dimensional solar-wind model that includes separate energy equations for the electrons and protons, proton temperature anisotropy, collisional and collisionless heat flux, and an analytical treatment of low-frequency, reflection-driven, Alfvén-wave (AW) turbulence. To partition the turbulent heating between electron heating, parallel proton heating, and perpendicular proton heating, we employ results from the theories of linear wave damping and nonlinear stochastic heating. We account for mirror and oblique firehose instabilities by increasing the proton pitch-angle scattering rate when the proton temperature anisotropy exceeds the threshold for either instability. We numerically integrate the equations of the model forward in time until a steady state is reached, focusing on two fast-solar-wind-like solutions. These solutions are consistent with a number of observations, supporting the idea that AW turbulence plays an important role in the origin of the solar wind.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ef418ad62882a1b6594b6c8b29d36344ab9113b7

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Citations in the corpus

The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere (2019, methodology): “Also plotted in Figure 6 are the flux ratios from two solutions of the solar wind model of Chandran et al. (2011).”
Nature of Kinetic Scale Turbulence in the Earth's Magnetosheath (2016, background): “For example, the fast solar wind model of Chandran et al. (2011) predicts βi ∼ 0.1 and βe ∼ 0.02 at 10 Solar radii from the Sun, a regime in which inertial kinetic Alfvén tur- bulence would be expected to constitute a significant fraction of the kinetic range.”
Slow Solar Wind: Observations and Modeling (2016, unknown): “Alternatively, for describing the heating terms one may invoke mechanisms based either on ion-cyclotron-resonance (see the review by Hollweg and Isenberg 2002) or on a perpendicular turbulent cascade (Chandran et al. 2011, and references therein).”
ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING (2013, methodology): “The stochastic heating parameter hs and the collisionless heat conduction parameter rH are assigned with the same values as in Chandran et al. (2011).”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “…1968; Hollweg 1986; Velli et al. 1991; Matthaeus et al. 1999; Suzuki and Inutsuka 2006; Cranmer et al. 2007; Ofman 2010; van Ballegooijen et al. 2011; Chandran et al. 2011; Matsumoto and Suzuki 2012; Perez and Chandran 2013; Lionello et al. 2014; Tenerani and Velli 2017; van Ballegooijen and…”
Electron Thermodynamics in GRMHD Simulations of Low-Luminosity Black Hole Accretion (2015, methodology): “A similar approach is often used in modeling the globa dynamics of the low-collisionality solar wind (e.g.,Chandran et al. 2011).”